Project Cyclops, A Design... - Department of Earth and Planetary ...
Project Cyclops, A Design... - Department of Earth and Planetary ...
Project Cyclops, A Design... - Department of Earth and Planetary ...
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lO II<br />
Substituting this relation into equation 5, Chapter 5,<br />
with Po = fiB we find the conventional range limit<br />
o<br />
t---<br />
iv.<br />
10 to<br />
w 109<br />
._1<br />
R<br />
- 4 _'-B I (9)<br />
q__ dr t1_)1/2 n I]4, n >> I (10)<br />
m<br />
er<br />
u_ 108<br />
0<br />
¢Y<br />
w<br />
en<br />
z<br />
107<br />
where<br />
dr = receiving antenna diameter<br />
Peff = Ptgt = effective radiated power<br />
= noise spectral density = kTat radio frequencies<br />
B = receiver b<strong>and</strong>width<br />
10 6<br />
I01<br />
10 2 I0 3 I0 4 I0 5<br />
ANTENNA<br />
DIAMETER<br />
r = integration time<br />
n = (Br)<br />
Figure 6-4.<br />
Number <strong>of</strong> resolvable directions versus<br />
diameter<br />
SEARCH RANGE LIMIT<br />
<strong>and</strong> wavelength.<br />
in radio astronomy <strong>and</strong> in most fields <strong>of</strong> measurement<br />
the minimum detectable signal amplitude is defined<br />
as being equal to the rms fluctuations due to noise.<br />
The signal-to-noise power ratio out <strong>of</strong> a square-law<br />
detector is given by equation (19) in Chapter 5 as<br />
where<br />
Pr = received signal power<br />
Po = noise power<br />
s ('°r/t'o)2<br />
--= n (7)<br />
N 1 + 2(Pr/Po)<br />
n = (Br) = number <strong>of</strong> independent samples that<br />
are averaged<br />
Setting SIN equal to unity we find for the received<br />
signal-to-noise<br />
ratio<br />
Pr 1 +x/rl-+ n<br />
-- = (8)<br />
Po<br />
n<br />
We use equation (119) in estimating range limits when<br />
the data processing system is unspecified. However, in<br />
determining the performance <strong>of</strong> the <strong>Cyclops</strong> system we<br />
use the actual range limit at which the probability <strong>of</strong><br />
missing the signal Pros <strong>and</strong> the probability <strong>of</strong> a false<br />
alarm Pfa have specified values. That is, we take<br />
draper f -- q ,/2<br />
R = -- f(n,Pms,Pr,) I (11)<br />
4_--_<br />
where f(n,Pms,Pfq) is evaluated for the proposed data<br />
processing method using the actual statistics, <strong>and</strong> will be<br />
a number on the order <strong>of</strong> unity. Anticipating this, we<br />
will use as a reference range limit for some <strong>of</strong> our curves<br />
the range Ro<br />
given by<br />
/ \I/2<br />
dr(Peff.<br />
4\/<br />
which is simply the range at which the received<br />
signal-to-noise ratio is unity <strong>and</strong> is less than R, as given<br />
by equation (9), for n > 3.<br />
DOPPLER SHIFTS AND RATES<br />
Relative motion between transmitter <strong>and</strong> receiver can<br />
occur because <strong>of</strong> (1) radial velocity <strong>of</strong> the star with respect<br />
to the Sun, (2) orbital velocity <strong>of</strong> the <strong>Earth</strong> <strong>and</strong><br />
I<br />
56